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Abstract Eruptive mass loss in massive stars is known to occur, but the mechanism(s) are not yet well understood. One proposed physical explanation appeals to opacity-driven super-Eddington luminosities in stellar envelopes. Here, we present a 1D model for eruptive mass loss and implement this model in theMESAstellar evolution code. The model identifies regions in the star where the energy associated with a local super-Eddington luminosity exceeds the binding energy of the overlaying envelope. The material above such regions is ejected from the star. Stars with initial masses of 10−100M_⊙at solar and SMC metallicities are evolved through core helium burning, with and without this new eruptive mass-loss scheme. We find that eruptive mass loss of up to ∼10⁻²M_⊙yr⁻¹can be driven by this mechanism, and occurs in a vertical band on the H-R diagram between $3.5\lesssim \log \left(T_{\mathrm{eff}}/\mathrm{K}\right)\lesssim 4.0$. This predicted eruptive mass loss prevents stars of initial masses ≳20M_⊙from evolving to become red supergiants (RSGs), with the stars instead ending their lives as blue supergiants, and offers a possible explanation for the observed lack of RSGs in that mass regime.